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Radio emission models of colliding-wind binary systems

Published online by Cambridge University Press:  26 May 2016

Sean M. Dougherty ,
Julian M. Pittard ,
Laura Kasian ,
Robert F. Coker ,
Peredur M. Williams  and
Huw Lloyd
Sean M. Dougherty
Affiliation:
NRC Dominion Radio Astrophysical Observatory, 717 White Lake Rd, Penticton, BC V2A 6K3, Canada
Julian M. Pittard
Affiliation:
Department of Physics and Astronomy, The University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
Laura Kasian
Affiliation:
NRC Dominion Radio Astrophysical Observatory, 717 White Lake Rd, Penticton, BC V2A 6K3, Canada
Robert F. Coker
Affiliation:
Los Alamos National Laboratory, X-2, MS P-225, Los Alamos, NM 87545, USA
Peredur M. Williams
Affiliation:
Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, Scotland, UK
Huw Lloyd
Affiliation:
Blade Interactive Studios, 274 Deansgate, Manchester M3 4JB, UK

Abstract

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We present preliminary calculations of the spatial distribution of the radio emission from a WR+OB colliding wind system, based on high-resolution hydrodynamical simulations and solutions to the radiative transfer equation. We account for both thermal and non-thermal radio emission, under the assumption of equipartition between magnetic and relativistic particle energy densities, and that the latter is a simple fraction of the thermal particle energy density. These calculations provide the foundation for modeling high resolution radio images and light curves of colliding-wind systems like WR 140, WR 146 and WR 147.

Type
Part 1. Atmospheres of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 170 - 171
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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